<i>Chandra</i>Observations of the Northeastern Rim of the Cygnus Loop

Katsuda, Satoru; Tsunemi, H.; Kimura, Masashi; Mori, Koji

doi:10.1086/588188

Cited by 23 publications

(33 citation statements)

References 36 publications

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“…A general finding is that single-temperature models and models based on time-dependent ionization behind a single shock do not provide adequate fits to Chandra, XMM-Newton, or Suzaku data (e.g., Katsuda et al 2008;Tsunemi et al 2007;Miyata et al 2007). They also tend to find depleted elemental abundances, even for elements such as oxygen that should not be depleted onto grains (Miyata et al 2007) and evidence for resonance line scattering (Miyata et al 2008).…”

Section: Previous Observations Of the Non-radiative Filamentmentioning

confidence: 99%

Dust Destruction in a Non-Radiative Shock in the Cygnus Loop Supernova Remnant

Sankrit

Williams

Borkowski

et al. 2010

ApJ

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We present 24 μm and 70 μm images of a non-radiative shock in the Cygnus Loop supernova remnant, obtained with the Multiband Imaging Photometer for Spitzer on board the Spitzer Space Telescope. The post-shock region is resolved in these images. The ratio of the 70 μm to the 24 μm flux rises from about 14 at a distance 0. 1 behind the shock front to about 22 in a zone 0. 75 further downstream, as grains are destroyed in the hot plasma. Models of dust emission and destruction using post-shock electron temperatures between 0.15 keV and 0.30 keV and post-shock densities, n H ∼ 2.0 cm −3 , predict flux ratios that match the observations. Non-thermal sputtering (i.e., sputtering due to bulk motion of the grains relative to the gas) contributes significantly to the dust destruction under these shock conditions. From the model calculations, we infer that about 35% by mass of the grains are destroyed over a 0.14 pc region behind the shock front.

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Section: Previous Observations Of the Non-radiative Filamentmentioning

confidence: 99%

Dust Destruction in a Non-Radiative Shock in the Cygnus Loop Supernova Remnant

Sankrit

Williams

Borkowski

et al. 2010

ApJ

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“…In addition, X-ray emissions from certain regions along northeast and southwest limbs have relatively high metal abundances also suggesting a high-mass, core-collapse supernova (Tsunemi et al 2007;Katsuda et al 2008;Kimura et al 2009;Uchida et al 2009;Fujimoto et al 2011;Katsuda et al 2011). Hubble (1937) of the bright eastern and western nebulae away from the centre of expansion.…”

Section: Introductionmentioning

confidence: 99%

A distance estimate to the Cygnus Loop based on the distances to two stars located within the remnant

Fesen

Neustadt

Black

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Underlying nearly every quantitative discussion of the Cygnus Loop supernova remnant is uncertainty about its distance. Here we present optical images and spectra of nebulosities around two stars whose mass-loss material appears to have interacted with the remnant's expanding shock front and thus can be used to estimate the Cygnus Loop's distance. Narrow passband images reveal a small emission-line nebula surrounding an M4 red giant near the remnant's eastern nebula NGC 6992. Optical spectra of the nebula show it to be shock-heated with significantly higher electron densities than seen in the remnant's filaments. This along with a bow-shaped morphology suggests it is likely red giant mass-loss material shocked and accelerated by passage of the Cygnus Loop's blast wave. We also identify a B7 V star located along the remnant's northwestern limb which also appears to have interacted with the remnant's shock wave. It lies within a small arc of nebulosity in an unusually complex region of highly curved and distorted filaments along the remnant's northern shock front suggestive of a localized disturbance of the shock front due to the B star's stellar winds. Based on the assumption that these two stars lie inside the remnant, combined with an estimated distance to a molecular cloud situated along the remnant's western limb, we propose a distance to the Cygnus Loop of 1.0 ± 0.2 kpc. Although larger than several recent estimates of 500 − 800 pc, a distance 1 kpc helps resolve difficulties with the remnant's postshock cosmic ray and gas pressure ratio and estimated supernova explosion energy.

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“…It also provides an electron-proton temperature ratio of >0.8, -6 -consistent with the determination of Ghavamian et al (2001) for a nearby position. In addition, the proper motions of the shocks in that region have been measured and the electron temperature is available from X-ray spectra (Salvesen et al 2009;Katsuda et al 2008). IR images from Spitzer and UV spectra from COS have been used to investigate the destruction of dust and the sputtering of carbon atoms from grains behind this shock (Sankrit et al 2010;Raymond et al 2013).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Carbon, Helium, and Proton Kinetic Temperatures in a Cygnus Loop Shock Wave

Raymond

Edgar

Ghavamian

et al. 2015

ApJ

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Observations of SN1006 have shown that ions and electrons in the plasma behind fast supernova remnant shock waves are far from equilibrium, with the electron temperature much lower than the proton temperature and ion temperatures approximately proportional to ion mass. In the ∼360 km s −1 shock waves of the Cygnus Loop, on the other hand, electron and ion temperatures are roughly equal, and there is evidence that the oxygen kinetic temperature is not far from the proton temperature. In this paper we report observations of the He II λ1640 line and the C IV λ1550 doublet in a 360 km s −1 shock in the Cygnus Loop. While the best fit kinetic temperatures are somewhat higher than the proton temperature, the temperatures of He and C are consistent with the proton temperature and the upper limits are 0.5 and 0.3 times the mass-proportional temperatures, implying efficient thermal equilibration in this collisionless shock. The equilibration of helium and hydrogen affects the conversion between proton temperatures determined from Hα line profiles and shock speeds, and that the efficient equilibration found here reduces the shock speed estimates and the distance estimate to the Cygnus Loop of Medina et al. (2014) to about 800 pc.

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ChandraObservations of the Northeastern Rim of the Cygnus Loop

Cited by 23 publications

References 36 publications

Dust Destruction in a Non-Radiative Shock in the Cygnus Loop Supernova Remnant

Dust Destruction in a Non-Radiative Shock in the Cygnus Loop Supernova Remnant

A distance estimate to the Cygnus Loop based on the distances to two stars located within the remnant

Carbon, Helium, and Proton Kinetic Temperatures in a Cygnus Loop Shock Wave

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